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1 Orbital Evidence for Clay and Acidic Sulfate Assemblages on Mars Based on 2 Mineralogical Analogs from Rio Tinto, Spain 3 4 Hannah H

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1 Orbital Evidence for Clay and Acidic Sulfate Assemblages on Mars Based on 2 Mineralogical Analogs from Rio Tinto, Spain 3 4 Hannah H 1 Orbital Evidence for Clay and Acidic Sulfate Assemblages on Mars Based on 2 Mineralogical Analogs from Rio Tinto, Spain 3 4 Hannah H. Kaplan1*, Ralph E. Milliken1, David Fernández-Remolar2, Ricardo Amils3, 5 Kevin Robertson1, and Andrew H. Knoll4 6 7 Authors: 8 9 1 Department of Earth, Environmental and Planetary Sciences, Brown University, 10 Providence, RI, 02912 USA. 11 12 2British Geological Survey, Nicker Hill, Keyworth, NG12 5GG, UK. 13 14 3 Centro de Astrobiologia (INTA-CSIC), Ctra Ajalvir km 4, Torrejon de Ardoz, 28850, 15 Spain. 16 17 4 Department of Organismic and Evolutionary Biology, Harvard University, 18 Çambridge, MA, USA. 19 20 *Corresponding author: [email protected] 1 21 Abstract 22 23 Outcrops of hydrated minerals are widespread across the surface of Mars, 24 with clay minerals and sulfates being commonly identified phases. Orbitally-based 25 reflectance spectra are often used to classify these hydrated components in terms of 26 a single mineralogy, although most surfaces likely contain multiple minerals that 27 have the potential to record local geochemical conditions and processes. 28 Reflectance spectra for previously identified deposits in Ius and Melas Chasma 29 within the Valles Marineris, Mars, exhibit an enigmatic feature with two distinct 30 absorptions between 2.2 – 2.3 µm. This spectral ‘doublet’ feature is proposed to 31 result from a mixture of hydrated minerals, although the identity of the minerals has 32 remained ambiguous. Here we demonstrate that similar spectral doublet features 33 are observed in airborne, field, and laboratory reflectance spectra of rock and 34 sediment samples from Rio Tinto, Spain. Combined visible-near infrared reflectance 35 spectra and X-ray diffraction measurements of these samples reveals that the 36 doublet feature arises from a mixture of Al-phyllosilicate (illite or muscovite) and 37 jarosite. Analyses of orbital data from the Compact Reconnaissance Imaging 38 Spectrometer for Mars (CRISM) shows that the martian spectral equivalents are also 39 consistent with mixtures of Al-phyllosilicates and jarosite, where the Al- 40 phyllosilicate may also include kaolinite and/or halloysite. A case study for a region 41 within Ius Chasma demonstrates that the relative proportions of the Al- 42 phyllosilicate(s) and jarosite vary within one stratigraphic unit as well as between 43 stratigraphic units. The former observation suggests that the jarosite may be a 44 diagenetic (authigenic) product and thus indicative of local pH and redox conditions, 2 45 whereas the latter observation may be consistent with variations in sediment flux 46 and/or fluid chemistry during sediment deposition. 47 48 Key points: 49 • A doublet absorption is observed in reflectance spectra of Mars between 2.2 - 50 2.3 µm. 51 • Reflectance spectra at Rio Tinto, Spain also show a doublet due to Al- 52 phyllosilicate and jarosite. 53 • Spectral variation in martian deposits suggests local variation in pH, redox, 54 and/or sediment flux. 55 56 57 Keywords: Mars, surface; Spectroscopy; Infrared observations 58 3 59 1. Introduction 60 Outcrops of sulfate and clay mineral-bearing rocks are widespread across 61 the ancient surface of Mars [Bibring et al., 2006; Murchie et al., 2009; Ehlmann et al., 62 2011; Carter et al., 2013], indicating that a complex history of water-rock interaction 63 is preserved in the martian rock record. Visible-near infrared (VIS-NIR) reflectance 64 spectra acquired by the CRISM (Compact Reconnaissance Imaging Spectrometer for 65 Mars) and OMEGA (Observatoire pour la Minéralogie, l’Eau, les Glaces et l’Activité) 66 imaging spectrometers have been used to identify clay minerals in ancient and 67 heavily cratered Noachian terrains [Poulet et al., 2005; Ehlmann et al., 2011; Carter 68 et al., 2013] and thick deposits of sulfates in younger Hesperian terrains and basins 69 [Gendrin et al., 2005; Bibring et al., 2006]. In the cases of Terra Meridiani, Gusev 70 Crater, and Gale Crater, these minerals have been examined in situ by rover-based 71 payloads, providing detailed local geologic context for some of these orbital 72 detections [e.g. Klingelhofer et al., 2004; Squyres et al., 2004; Arvidson et al., 2008; 73 Wang et al., 2006; Vaniman et al., 2014]. 74 75 Many of these orbiter-based detections of hydrated minerals on Mars are 76 discussed in terms of single minerals. That is, the reflectance spectra of these 77 deposits are commonly discussed or interpreted as specific clay, sulfate, or other 78 hydrated minerals (see Ehlmann et al., 2009 for an exception with regards to 79 mineral assemblages at Nili Fossae). Though these deposits are undoubtedly 80 polymineralic, it appears that in many cases a single mineral can be spectrally 81 dominant even at the spatial resolution of instruments such as CRISM (e.g., ~18 4 82 m/pixel). Therefore, those regions on Mars whose reflectance spectra cannot clearly 83 be attributed to a single dominant hydrated mineral are of particular interest as 84 they may record different and more diverse geological processes than are typically 85 recognized from CRISM data. 86 87 Reflectance spectra of deposits and strata within the Valles Marineris reveal 88 a number of locations that fall within this category, and these are the focus of this 89 study. Specifically, CRISM spectra of various deposits within Ius, Melas, and other 90 chasmata exhibit an absorption feature with local minima centered at ~2.21 and 91 ~2.27 μm [Metz et al., 2009; Roach et al., 2010; Weitz et al., 2011] (Figure 1). The 92 spectral shape and properties of this absorption feature, which we will refer to as a 93 spectral ‘doublet’, does not match the spectrum of any single common mineral in 94 existing spectral libraries, suggesting it likely cannot be attributed to a single type of 95 clay, sulfate, or other common hydrated mineral. 96 97 Previous studies have hypothesized that this material represents a mixture 98 of clays, sulfates (possibly including jarosite), and/or poorly crystalline phases 99 [Roach et al., 2010; Tosca et al., 2008b; Noe Dobrea et al., 2011; Weitz et al., 2014], 100 but the exact assemblage remains unknown. We have observed that similar spectral 101 features occur in airborne, field, and lab spectra of rocks and sediments at Rio Tinto, 102 Spain, which has been previously studied as a Mars analog due to the river’s acidity, 103 iron hydrochemistry, and extensive iron oxide deposits [Fernandez-Remolar et al. 104 2003]. Indeed, it has been suggested that the ferric iron and sulfate mineralogy 5 105 produced by the acidic waters may be analogous to conditions experienced in Terra 106 Meridiani during the Hesperian [Fernandez-Remolar et al., 2004], and similar 107 conditions may also have occurred in portions of the Valles Marineris [e.g., Bibring 108 et al., 2007]. 109 110 In this study we integrate airborne, in situ, and lab measurements to 111 characterize a suite of samples from different sites at Rio Tinto to understand the 112 mineralogical origin of the ‘doublet’ spectral signature, and we then compare our 113 findings to reflectance spectra acquired by the CRISM instrument for deposits in 114 Valles Marineris, Mars. We demonstrate that the doublet absorptions observed in 115 samples from Rio Tinto are comparable to the spectral signatures observed in Valles 116 Marineris, that the former are the result of Al-bearing phyllosilicates mixed with 117 jarosite, and that similar mineral assemblages may be present on Mars. This 118 indicates Rio Tinto contains materials that can serve as mineralogical and spectral 119 analogs for the martian deposits, though the geological processes that lead to the 120 formation of these assemblages on Earth and Mars need not be equivalent. 121 Specifically, although jarosite and Al-phyllosilicates may co-occur in geologic units 122 today on Mars, this association does not require their formation environments to 123 have been the same in space and/or time. Both mineral types may be authigenic or 124 detrital, and detailed geologic context is necessary to distinguish between these 125 options and the associated implications for local paleoenvironmental conditions. 126 127 2. Background 6 128 2.1 Overview of Clay and Sulfate Detections on Mars 129 The most commonly observed spectral signatures on Mars that have been 130 interpreted as clay minerals are identified as Fe/Mg smectite, but mixed-layer clays, 131 chlorite, Al-smectite, mica, kaolinite, and serpentine have also been observed 132 [Mustard et al., 2008; Murchie et al., 2009; Ehlmann et al., 2011; Carter et al., 2013]. 133 Aqueous alteration of basaltic protoliths both at the surface and in the subsurface 134 have been invoked as the major source of these clay minerals, although subsequent 135 erosion and eolian/fluvial transport has led to their occurrence in a number of 136 different depositional environments. Intriguingly, these clay minerals, hereafter 137 referred to simply as ‘clays’, occur predominantly in terrains that are Noachian 138 (>3.6 Ga) in age [Bibring et al., 2006]. The presence and apparent spatial and 139 temporal distribution of these clays has been used to infer that early Mars was 140 characterized by circum-neutral pH, low salinity, and possibly habitable conditions 141 [Ehlmann et al., 2011]. More recently, in situ observations of clay-bearing 142 mudstones in Gale Crater by the Curiosity rover are also supportive of a habitable 143 environment, possibly during the Hesperian [Grotzinger et al., 2014; 2015; Vaniman 144 et al., 2014; Bristow et al., 2015]. 145 146 In contrast, sulfate detections on Mars typically occur in younger Hesperian 147 terrains and may be indicative of a decreased hydrological cycle [Bibring et al., 148 2006]. Decreased water availability, coupled with increasing salinity, may indicate 149 near-surface conditions inhospitable to most life [e.g., Tosca et al., 2008a].
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